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THE SILICON AND CALCIUM HIGH-VELOCITY FEATURES IN TYPE Ia SUPERNOVAE FROM EARLY TO MAXIMUM PHASES
Zhao, XL1,2; Wang, XF1; Maeda, K2,3; Sai, H1; Zhang, TM4; Zhang JJ(张居甲)5,6; Huang, F1,7; Rui, LM1; Zhou, Q1; Mo, J1
Source PublicationASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
2015-09
Volume220Issue:1
DOI10.1088/0067-0049/220/1/20
Contribution Rank第5完成单位
Indexed BySCI
KeywordMethods: Data Analysis Supernovae: General Techniques: Spectroscopic
Abstract

The high-velocity features (HVFs) in optical spectra of type Ia supernovae (SNe Ia) are examined with a large sample including very early-time spectra (e.g., t < -7 days). Multiple Gaussian fits are applied to examine the HVFs and their evolutions, using constraints on expansion velocities for the same species (i.e., Si II 5972 and Si II 6355). We find that strong HVFs tend to appear in SNe Ia with smaller decline rates (e.g., Delta m(15)(B) less than or similar to 1.4 mag), clarifying that the finding by Childress et al. for the Ca-HVFs in near-maximum-light spectra applies both to the SiHVFs and Ca-HVFs in the earlier phase. The Si-HVFs seem to be more common in rapidly expanding SNe Ia, which is different from the earlier result that Ca-HVFs are associated with SNe Ia that have slower Si II 6355 velocities at maximum light (i.e., V-max(Si)). Moreover, SNe Ia with both stronger HVFs at early phases and larger V-max(Si) are found to have noticeably redder B - V colors and to occur preferentially in the inner regions of their host galaxies, while those with stronger HVFs but smaller V-max(Si) show opposite tendencies, suggesting that these two subclasses have different explosion environments and their HVFs may have different origins. We further examine the relationships between the absorption features of Si II 6355 and Ca II IR lines, and find that their photospheric components are well correlated in velocity and strength but that the corresponding HVFs show larger scatter. These results cannot be explained with ionization and/or thermal processes alone, and different mechanisms are required for the creation of HVF-forming regions in SNe Ia.

Funding ProjectMajor State Basic Research Development Program[2013CB834903] ; National Natural Science Foundation of China (NSFC)[11178003] ; National Natural Science Foundation of China (NSFC)[11325313] ; China Scholarship Council (CSC)[201406210312] ; Chinese Academy of Sciences[XDB09000000] ; JSPS[26800100] ; World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan ; People's Government of Yunnan Province ; US National Science Foundation[AST 0907903] ; CAS
Funding OrganizationMajor State Basic Research Development Program[2013CB834903] ; National Natural Science Foundation of China (NSFC)[11178003, 11325313] ; China Scholarship Council (CSC)[201406210312] ; Chinese Academy of Sciences[XDB09000000] ; JSPS[26800100] ; World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan ; People's Government of Yunnan Province ; US National Science Foundation[AST 0907903] ; CAS
Language英语
Subject Area天文学 ; 恒星与银河系 ; 恒星天文学
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherIOP PUBLISHING LTD
Publication PlaceTEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN0067-0049
URL查看原文
WOS IDWOS:000364049900020
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordDELAYED-DETONATION MODELS ; PHOTOMETRY DATA RELEASE ; WHITE-DWARF MODELS ; BVRI LIGHT CURVES ; SN 2011FE ; CIRCUMSTELLAR MATERIAL ; SPECTROSCOPIC DIVERSITY ; OPTICAL SPECTROSCOPY ; 3-DIMENSIONAL MODELS ; INFRARED PHOTOMETRY
Citation statistics
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/5457
Collection丽江天文观测站(南方基地)
中国科学院天体结构与演化重点实验室
Corresponding AuthorZhao, XL
Affiliation1.Center for Astrophysics, Department of Physics, Tsinghua University, Beijing, 100084, China
2.Department of Astronomy, Kyoto University, Kyoto, 606-8502, Japan
3.Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, Japan
4.National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
5.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, China
6.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, China
7.Department of Astronomy, Beijing Normal University, Beijing 100875, China
Recommended Citation
GB/T 7714
Zhao, XL,Wang, XF,Maeda, K,et al. THE SILICON AND CALCIUM HIGH-VELOCITY FEATURES IN TYPE Ia SUPERNOVAE FROM EARLY TO MAXIMUM PHASES[J]. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES,2015,220(1).
APA Zhao, XL.,Wang, XF.,Maeda, K.,Sai, H.,Zhang, TM.,...&Mo, J.(2015).THE SILICON AND CALCIUM HIGH-VELOCITY FEATURES IN TYPE Ia SUPERNOVAE FROM EARLY TO MAXIMUM PHASES.ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES,220(1).
MLA Zhao, XL,et al."THE SILICON AND CALCIUM HIGH-VELOCITY FEATURES IN TYPE Ia SUPERNOVAE FROM EARLY TO MAXIMUM PHASES".ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES 220.1(2015).
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